Towards a better dynamic theory for type III radio bursts

An approximate numerical solution is given to the quasilinear equations governing the interaction of the electron streams exciting type III solar radio bursts and the background plasma. The density and temperature variations are taken into account and the stream is studied from r =1 to 20 R. The method used is to level any positive slopes in the distribution function as they develop and record the energy released. None of the energy released is allowed to return to the stream and since no other damping mechanisms are taken into account, the solution is only applicable to the initial rise of the burst. Even then, the solution gives more decleration of the leading edge of the burst than observed which indicates that letting some of the energy released return to the stream is necessary. At the same time the solution does show that depletion of high velocity electrons is an important process and calls into question any analysis which neglects this process by, for example, integrating over the spectrum of plasma waves such as Zaitsev et al. (1972). It is shown that the case considered here is an opposite limiting case to the one considered by Zaitsev et al. and what needs to be done to find the more realistic solution in between these two limiting cases is indicated.The National Center for Atmospheric Research is sponsored by the National Science Foundation.